As this was an eclipse observation, longer exposure aperture synthesis was considered unsuitable. Snapshot imaging was used instead and in order to increase the \(u,v\)  coverage, multi-frequency synthesis (MFS) was implemented [1]}, [2]}, [3]}. The visibilities at several frequencies were concatenated into a multi-frequency band. A number of iterations of self-calibration were then applied using a multiscale, multi-frequency synthesis (MS-MFS) CLEAN [4]}, [5]}. MFS is a useful technique to increase \(u,v\)  coverage without the inclusion of additional baselines. fig:figure2 demonstrates that for a particular baseline it is possible to have many \(u,v\)  points corresponding to different frequencies. For this work a frequency range of 120–180 MHz was divided into three separate multi-frequency bands; 120–140 MHz, 140–160 MHz, and 160–180 MHz. Each band has a width of 20 MHz as the spectral brightness of the radio non-flaring Sun is known not to vary greatly over this range at these frequencies.
